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On the Temporal Relationship between Coronal Mass Ejections and Flares

  • Authors: J. Zhang, K. P. Dere, R. A. Howard, M. R. Kundu, and S. M. White

Zhang et al. 2001 The Astrophysical Journal 559 452.

  • Provider: AAS Journals

Caption: Fig. 2.

Upper panel: height‐time profile (dotted line) of the CME on 1998 June 11 vs. the temporal profile of GOES X‐ray flux of corresponding M1.4 flare (solid line). The Y‐axis denotes the CME height (heliocentric distance of CME front in units of ﹩R_{\odot }﹩), and the X‐ray flux is displayed as an arbitrary unit. The CME heights, which are measured in a set of LASCO C1, C2, and C3 images are designated by asterisks, triangles, and squares, respectively; the dotted line connects these symbols. Lower panel: CME velocity‐time profile (dotted line) vs. the flare temporal profile (solid line). Velocities are derived using the height difference between the images at the given time and the previous image.

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